Finally, the PNS-fallback disk system has also been invoked to explain the light curve of luminous and extreme SNe of types Ib/c [1]}, [2]}, [3]}. We may also expect our scenario to produce these types of explosions depending on the amount of accreted mass during the dynamo process. First, PNSs that have accreted \(\sim {2}{}-{3e-2}{M_{\odot }}\)  of fallback matter before the magnetic field saturation have rotation periods around \(\sim {10}{}-{20}{ms}\) , which are too slow to produce extreme explosions. According to our scenario, their typical magnetic field is of \({1}{}-{5e14}{G}\) , which would lead to regular luminous SNe Ib/c. Their light curve would be dominated by the PNS spin-down luminosity instead of the \(^{56}\) Ni decay luminosity [4]}, [5]}. Second, for fallback masses spinning up the PNSs to millisecond rotation periods, the magnetic field saturates a few \({10}{s}\)  after the core bounce at \(B_r\gtrsim {5e14}{G}\) . The rotational energy can be kept for later times and be slowly extracted to irradiate its environment, which might lead to superluminous SNe I [6]}, [7]}, [8]}, [9]}, [10]}, [3]}. Finally, to produce extreme explosions such as hypernovae, which have \(\sim 10\)  times larger kinetic energies and much higher \(^{56}\) Ni yields than the far majority of CCSNe, an energy injection within a timescale of \(\lesssim {1}{s}\)  is required [12]} to explain the large masses of \(^{56}\) Ni \(\gtrsim {0.2}{M_{\odot }}\)  inferred from their light curve [13]}, [14]}, [15]}. For rotation periods of \(\lesssim {1}{ms}\) , which correspond to rotational energies of \(\gtrsim {3e52}{erg}\) , our model provides a radial magnetic field of \(B_r\gtrsim {2.6e16}{G}\) , which may be enough to inject the energy quickly through magnetic dipole spin-down only [16]}. The presence of a propeller regime would enhance the PNS spin-down such that a weaker dipolar magnetic field of \(\sim {2e15}{G}\)  field would also produce a hypernova [2]} but through a propeller-powered explosion. Therefore, our magnetic field amplification scenario by PNS accretion or fallback accretion may be of relevance for a wide variety of magnetar-powered phenomena in different types of SN events.
